Mathematics – Logic
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21111103c&link_type=abstract
American Astronomical Society, AAS Meeting #211, #111.03; Bulletin of the American Astronomical Society, Vol. 39, p.940
Mathematics
Logic
Scientific paper
Stellar feedback is the most difficult ingredient in galaxy formation models. The basic idea is that massive stars inject energy, mass and metals back to the interstellar medium(ISM) through stellar winds and supernova explosions. Although this injection happens at scales bellow 100 pc, it affects the ISM and galaxy formation. We use cosmological N-body+Hydrodynamics simulations of galaxy formation, as well as simulations of the ISM to study the effect of stellar feedback on galactic scales. Stellar feedback maintains gas with temperatures above a million degrees. This gas fills bubbles, super-bubbles and chimneys. It is also crucial to understand where and how the energy from massive stars is released back to the ISM. While a large fraction of massive stars in our Galaxy are found in stellar clusters, 10-30% are found in the field with high peculiar velocities (Gies 1987). Besides the significant fraction of this runaway stars, little attention has been paid to their effect on galaxy formation. We model runaway stars by adding a random velocity to 10%-30% of the stellar particles, so %10 of runaway stars have peculiar velocities higher than 40 Km /s. We first study the effect of stellar feedback in the ISM, using simulations of a 4 Kpc piece of the ISM with a 14 pc resolution. Then, we check whether this picture holds when the resolution is degraded to the resolution that our cosmological simulations can achieve at high redshift. We find that only if the effect of runaway stars is included and the resolution is better than 50 pc, the hot phase of the ISM can be reproduced. This is 10 times better than the typical resolution in cosmological simulations of galaxy formation. Only with this resolution, the effect of stellar feedback in galaxy formation is resolved without any assumption about sub-resolution physics.
Ceverino-Rodriguez Daniel M.
Klypin Anatoly
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